As massas das duas estrelas de naªutrons em colisão são diferentes o suficiente, a companheira maior rasga a menor. Isso causa uma fusão mais lenta que permite que um
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)
Atravanãs de uma sanãrie de simulações, uma equipe internacional de pesquisadores determinou que algumas fusaµes de estrelas de naªutrons produzem radiação que deve ser detecta¡vel da Terra. Quando as estrelas de naªutrons de massa desigual se fundem, a estrela menor éarrancada pelas forças da maréde seu companheiro macia§o (a esquerda).
A maior parte da massa do parceiro menor cai sobre a estrela massiva, causando o colapso e a formação de um buraco negro (meio). Mas parte do material éejetada no Espaço; o resto recua para formar um enorme disco de acreção ao redor do buraco negro (a direita). Crédito da figura: Adaptado da figura 4 em "Formação imediata de buraco negro induzido pela acreção em fusaµes assimanãtricas de estrelas de naªutrons, sinais dina¢micos de ejetos e kilonova". Crédito: Bernuzzi et al., Avisos mensais da Royal Astronomical Society.
Quando duas estrelas de naªutrons se chocam, o resultado a s vezes éum buraco negro que engole tudo, exceto as evidaªncias gravitacionais da colisão. No entanto, em uma sanãrie de simulações, uma equipe internacional de pesquisadores, incluindo um cientista da Penn State, determinou que essas colisaµes normalmente silenciosas - pelo menos em termos de radiação que podemos detectar na Terra - a s vezes podem ser muito mais barulhentas.
"Quando duas estrelas de naªutrons incrivelmente densas e colapsadas se combinam para formar um buraco negro, fortes ondas gravitacionais emergem do impacto", disse David Radice, professor assistente de física e astronomia e astrofasica da Penn State e membro da equipe de pesquisa. "Agora podemos captar essas ondas usando detectores como LIGO nos Estados Unidos e Virgo na Ita¡lia. Um buraco negro tipicamente engole qualquer outra radiação que possa ter surgido da fusão que poderaamos detectar na Terra, mas atravanãs de nossa simulações, descobrimos que esse nem sempre éo caso ".
A equipe de pesquisa descobriu que, quando as massas das duas estrelas de naªutrons em colisão são diferentes o suficiente, a companheira maior rasga a menor. Isso causa uma fusão mais lenta que permite que um "estrondo" eletromagnético escape. Os astrônomos devem ser capazes de detectar esse sinal eletromagnanãtico, e as simulações fornecem assinaturas dessas colisaµes barulhentas que os astrônomos poderiam procurar na Terra.
"Para entendaª-los, temos que simular muitos modelos possaveis para ver quais são compataveis com observações astrona´micas. Uma única simulação de um modelo não nos diria muito; precisamos realizar um grande número de simulações bastante computacionalmente intensivas. precisam de uma combinação de alta capacidade e alta capacidade que somente ma¡quinas como a Bridges podem oferecer. Esse trabalho não seria possível sem o acesso a esses recursos nacionais de supercomputação ".
A equipe de pesquisa, que inclui membros da colaboração internacional CoRe (Computational Relativity), descreve suas descobertas em um artigo publicado on-line no mensais da Royal Astronomical Society .
"Recentemente, a LIGO anunciou a descoberta de um evento de fusão no qual as duas estrelas tem massas possivelmente muito diferentes", disse Radice. "A principal consequaªncia nesse cena¡rio éque esperamos essa contrapartida eletromagnanãtica muito característica do sinal da onda gravitacional."
Depois de relatar a primeira detecção de uma fusão de estrelas de naªutrons em 2017, em 2019, a equipe do LIGO relatou a segunda, que eles chamaram de GW190425. O resultado da colisão de 2017 foi sobre o que os astrônomos esperavam, com uma massa total de cerca de 2,7 vezes a massa do nosso sol e cada uma das duas estrelas de naªutrons aproximadamente iguais em massa. Mas o GW190425 era muito mais pesado, com uma massa combinada de cerca de 3,5 massas solares e a proporção dos dois participantes mais desiguais - possivelmente tão alta quanto 2 para 1.
"Embora uma diferença de 2 para 1 na massa possa não parecer uma grande diferença, apenas uma pequena faixa de massas épossível para estrelas de naªutrons", disse Radice.
As estrelas de naªutrons podem existir apenas em uma faixa estreita de massas entre cerca de 1,2 e 3 vezes a massa do nosso sol. Remanescentes estelares mais leves não colapsam para formar estrelas de naªutrons e formam ana£s brancas, enquanto objetos mais pesados ​​colapsam diretamente para formar buracos negros . Quando a diferença entre as estrelas em fusão étão grande quanto em GW190425, os cientistas suspeitam que a fusão possa ser mais confusa - e mais alta em radiação eletromagnanãtica. Os astrônomos não haviam detectado esse sinal na localização de GW190425, mas a cobertura daquela área do canãu por telesca³pios convencionais naquele dia não era boa o suficiente para descarta¡-lo.
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Para entender o fena´meno de colisão de estrelas de naªutrons desiguais e para prever assinaturas de colisaµes que os astrônomos poderiam procurar, a equipe de pesquisa realizou uma sanãrie de simulações usando a plataforma Bridges do Pittsburgh Supercomputing Center e a plataforma Comet do San Diego Supercomputer Center - ambas na National Rede XSEDE da Science Foundation de centros e computadores de supercomputação - e outros supercomputadores.
Os pesquisadores descobriram que, como as duas estrelas simuladas de naªutrons espiralavam uma em direção a outra, a gravidade da estrela maior despedaço u seu parceiro. Isso significava que a estrela menor de naªutrons não atingiu seu companheiro mais macia§o de uma são vez. O despejo inicial da matéria da estrela menor transformou a maior em um buraco negro. Mas o restante de sua matéria estava muito longe para o buraco negro capturar imediatamente. Em vez disso, a chuva mais lenta da matéria no buraco negro criou um flash de radiação eletromagnanãtica.
A equipe de pesquisa espera que a assinatura simulada que eles encontraram possa ajudar os astrônomos usando uma combinação de detectores de ondas gravitacionais e telesca³pios convencionais a detectar os sinais emparelhados que anunciam o rompimento de uma estrela menor de naªutrons que se funde com uma maior.
As simulações exigiram uma combinação incomum de velocidade de computação, grandes quantidades de memória e flexibilidade na movimentação de dados entre memória e computação. A equipe usou cerca de 500 núcleos de computação, executando semanas a fio, em cerca de 20 insta¢ncias separadas. As muitas quantidades físicas que precisavam ser contabilizadas em cada ca¡lculo exigiam cerca de 100 vezes mais memória que uma simulação astrofasica tapica.
"Ha¡ muita incerteza em torno das propriedades das estrelas de naªutrons ", disse Radice. "Para entendaª-los, temos que simular muitos modelos possaveis para ver quais são compataveis com observações astrona´micas. Uma única simulação de um modelo não nos diria muito; precisamos realizar um grande número de simulações bastante computacionalmente intensivas. precisam de uma combinação de alta capacidade e alta capacidade que somente ma¡quinas como a Bridges podem oferecer. Esse trabalho não seria possível sem o acesso a esses recursos nacionais de supercomputação ".